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On the Particle-Size Distribution Function of Cometary Dust

Published online by Cambridge University Press:  14 August 2015

Z. Sekanina
Z. Sekanina*
Affiliation:
Harvard-Smithsonian Center for Astrophysics Cambridge, Massachusetts, U.S.A.

Extract

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The Finson-Probstein (1968a) method of analysis of the distribution of light intensity in dust tails has so far been applied to only a handful of comets. Yet, the results already suggest a striking diversity in the properties of the particle-size related distribution function f(β), one of three parametric functions determined. Here β is the acceleration exerted on the particle by solar radiation pressure, measured in units of solar attraction. For a spherical particle β is a function of its radius a, density ρ, and the integrated efficiency factor for radiation pressure Qpr (i.e., the ratio of the particle's effective cross-section for radiation pressure to its geometric cross-section): where c0 = 0.585 × 10−4 g/cm2.

Type
III: The Interplanetary Dust Complex 1. Sources, Evolution, and Dynamics
Information
Symposium - International Astronomical Union , Volume 90: Solid Particles in the Solar System , 1980 , pp. 251 - 254
Copyright
Copyright © Reidel 1980 

References

Finson, M. L. and Probstein, R. F.: 1968a, Astrophys. J. 154, pp. 327–352.Google Scholar
Finson, M. L. and Probstein, R. F.: 1968b, Astrophys. J. 154, pp. 353–380.Google Scholar
Jambor, B. J.: 1973, Astrophys. J. 185, pp. 727–734.Google Scholar
Sekanina, Z.: 1980, review paper in this volume.Google Scholar
Sekanina, Z. and Miller, F. D.: 1973, Science 179, pp. 565–567.CrossRefGoogle Scholar